A.P. Lobanov, J.A. Zensus, C. Cesarsky, Ph. Diamond's Exploring the Cosmic Frontier: Astrophysical Instruments for PDF

By A.P. Lobanov, J.A. Zensus, C. Cesarsky, Ph. Diamond

ISBN-10: 3540397558

ISBN-13: 9783540397557

ISBN-10: 3540397566

ISBN-13: 9783540397564

On may well 18-21, 2004, the Max-Planck-Society’s Harnack-Haus in Dahlem, Berlin hosted the foreign symposium "Exploring the Cosmic Frontier: Astrophysical tools for the twenty first Century". The symposium used to be devoted to exploring the complementarity and synergies among various branches of astrophysical learn, by means of featuring and discussing the basic clinical difficulties that would be addressed within the following few many years.

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Optical and Near-IR Facilities 29 At ten times the combined collecting area of every telescope ever built, a 100m filled aperture telescope would open new horizons in observational astronomy – going from 10m to 100m represents a “quantum” jump similar to that from the naked eye to Galileo’s telescope. Simulations show that V=38 point sources can be detected in 10 hours assuming diffraction-limited quality, more than a 1000-fold improvement over the VLT. OWL is very complementary to JWST. 5 µm and spectrography (R ≥ 5, 000) at λ < 5 µm.

Instruments designed for a seeing-limited 100-m would be impossibly large or wholly inefficient or both. g. a mosaic of multi-band imagers, but none covering core OWL science cases. The price to pay to get efficient instruments is of course the exacting adaptive optics system which must be incorporated in the overall concept right from the start. Optical and Near-IR Facilities 29 At ten times the combined collecting area of every telescope ever built, a 100m filled aperture telescope would open new horizons in observational astronomy – going from 10m to 100m represents a “quantum” jump similar to that from the naked eye to Galileo’s telescope.

G. Protheroe [14]. These high energy neutrinos produce an observable pulse of Cherenkov emission at radio frequencies if they interact in the front surface of the moon [15]. A patch of SKA antennas operating in the continuum between 1–2 GHz could be configured to detect such pulses with sensitivity 3 orders of magnitude better than any existing experiment [16,17]. 4 Observing Transients Before They Happen Entirely new ways of doing astronomy may be possible with the SKA. With an array that is pointed electronically, the raw, ‘undetected’ signals can be recorded in memory.

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Exploring the Cosmic Frontier: Astrophysical Instruments for the 21st Century (ESO Astrophysics Symposia) by A.P. Lobanov, J.A. Zensus, C. Cesarsky, Ph. Diamond


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